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Magnetic structures of an emerging flux region in the solar photosphere and chromosphere
Xu Z(徐稚)1,2; Lagg, A1; Solanki, SK1,3; Xu, Z (reprint author), Max Planck Inst Sonnensyst Forsch, Max Planck Str 2, D-37191 Katlenburg Lindau, Germany.
Source PublicationASTRONOMY & ASTROPHYSICS
2010-09
Volume520
DOI10.1051/0004-6361/200913227
Contribution Rank第2完成单位
Indexed BySCI ; EI
KeywordMagnetic Fields Sun: Chromosphere Sun: Infrared
AbstractAims. We investigate the vector magnetic field and Doppler velocity in the photosphere and upper chromosphere of a young emerging flux region of the sun close to disk center. Methods. Spectropolarimetric scans of a young active region made using the second generation Tenerife Infrared Polarimeter (TIP II) on the German Vacuum Tower Telescope (VTT) are analyzed. The scanned area contained multiple sunspots and an emerging flux region. An inversion based on the Milne-Eddington approximation was performed on the full Stokes vector of the chromospheric He I 10 830 angstrom and the photospheric Si I 10 827.1 angstrom lines. This provided the magnetic vector and line-of-sight velocity at each spatial point in both atmospheric layers. Results. A clear difference is seen between the complex magnetic structure of the emerging flux region (EFR) in the photosphere and the much simpler structure in the upper chromosphere. The upper chromospheric structure is consistent with a set of emerging loops following elongated dark structures seen in the He I 10 830 angstrom triplet, similar to arch filament systems (AFS), while in the photosphere we infer the presence of U-loops within the emergence zone. Nonetheless, in general the upper chromospheric field has a similar linear relationship between inclination angle and field strength as the photospheric field: the field is weak (approximate to 300 G) and horizontal in the emergence zone, but strong (up to 850 G) and more vertical near its edges. The field strength decreases from the photosphere to the upper chromosphere by approximately 0.1-0.2 Gkm(-1) (or even less) within the emergence zone and by 0.3-0.6 Gkm(-1) in sunspots located at its edge. We reconstructed the magnetic field in 3D based on the chromospheric vector field under the assumption that the He I 10 830 angstrom triplet forms along the magnetic field loops. The reconstructed loops are quite flat with supersonic downflows at both footpoints. Arguments and evidence for an enhanced formation height of He I 10 830 angstrom in arch-filaments seen in this line are provided, which support the validity of the reconstructed loops. Conclusions. The main chromospheric properties of EFRs previously deduced for a single region NOAA 9451 are shown to be valid for another region as well, suggesting that the main original results may have a wider application. The main exception is that only the first region displayed a current sheet in the chromosphere. We propose a scenario in which the relatively complex photospheric structure evolves into the simpler chromospheric one.
Funding OrganizationNational Natural Science Foundation of China [10933003] ; Korean Ministry of Education, Science and Technology [R31-10016]
Language英语
Subject AreaAstronomy & Astrophysics
SubtypeArticle
ISSN0004-6361
URL查看原文
WOS IDWOS:000283064200099
WOS Research AreaAstronomy & Astrophysics
WOS SubjectAstronomy & Astrophysics
WOS KeywordI 10830 ANGSTROM ; HIGH-RESOLUTION SPECTROSCOPY ; HEI LAMBDA-10830 MULTIPLET ; ARCH FILAMENT SYSTEMS ; STOKES PROFILES ; ACTIVE-REGION ; CONVECTION ZONE ; VECTOR ; FIELDS ; LINE
Citation statistics
Cited Times:22[WOS]   [WOS Record]     [Related Records in WOS]
Document Type期刊论文
Identifierhttp://ir.ynao.ac.cn/handle/114a53/6161
Collection太阳物理研究组
Corresponding AuthorXu, Z (reprint author), Max Planck Inst Sonnensyst Forsch, Max Planck Str 2, D-37191 Katlenburg Lindau, Germany.
Affiliation1.Max-Planck-Institut für Sonnensystemforschung, Max-Planck-Strasse 2, 37191 Katlenburg-Lindau, Germany
2.Yunnan Astronomical Observatory/National Astronomical Observatories, Chinese Academy of Science, Kunming 650011, PR China
3.School of Space Research, Kyung Hee University, Yongin, Gyeonggi 446-701, Korea
First Author AffilicationYunnan Observatories, Chinese Academy of Sciences
Recommended Citation
GB/T 7714
Xu Z,Lagg, A,Solanki, SK,et al. Magnetic structures of an emerging flux region in the solar photosphere and chromosphere[J]. ASTRONOMY & ASTROPHYSICS,2010,520.
APA Xu Z,Lagg, A,Solanki, SK,&Xu, Z .(2010).Magnetic structures of an emerging flux region in the solar photosphere and chromosphere.ASTRONOMY & ASTROPHYSICS,520.
MLA Xu Z,et al."Magnetic structures of an emerging flux region in the solar photosphere and chromosphere".ASTRONOMY & ASTROPHYSICS 520(2010).
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